A5030468255- Planetary Science and Exploration
- Astro and Planetary Science
- Space Science and Extraterrestrial Life
- Space Exploration and Technology
- Spaceflight effects on biology
- Geomagnetism and Paleomagnetism Studies
- Atmospheric and Environmental Gas Dynamics
- Solar and Space Plasma Dynamics
- Atmospheric Ozone and Climate
- Astronomy and Astrophysical Research
- Laser-induced spectroscopy and plasma
- Space Satellite Systems and Control
- Stellar, planetary, and galactic studies
Laboratory for Atmospheric and Space Physics
2022-2024
University of Colorado Boulder
2022-2024
Khalifa University of Science and Technology
2022-2024
University of Colorado System
2023-2024
University of California, Berkeley
2024
Abstract We present the first observations of dayside coronal oxygen emission in far ultraviolet (FUV) measured by Emirates Mars Ultraviolet Spectrometer (EMUS) onboard Mission (EMM). The high sensitivity EMUS is providing an opportunity to observe tenuous corona FUV, which otherwise difficult observe. Oxygen resonance fluorescence at 130.4 nm provides a measurement upper atmospheric and exospheric oxygen. More than 500 profiles are constructed using long–exposure time cross–exospheric mode...
Abstract We present the first measurements of Mars discrete aurora in extreme ultraviolet (<110 nm) and synoptic images far (110–180 nm). Auroral emission is detected >75% nightside images, with patterns shifting visibly over 15–20 min. Aurora observed most frequently regions open magnetic topology (where crustal fields are very weak and/or vertical), brightest where strongest. disk‐averaged spectrum aurora, several O, C, CO features as expected for electron impact primarily on 2 ....
Abstract Proton aurora at Mars are thought to form indirectly, as a result of solar wind proton charge exchange with planetary coronal hydrogen upstream the bow shock. This produces beamed energetic neutral atoms that bypass induced magnetosphere and cause spatially uniform auroral emission when they collide thermosphere. Here we report multiple definitive observations localized “patchy” using Emirates Ultraviolet Spectrometer on Mission, characterize plasma environment during these events...
Abstract We examine the newly discovered phenomena of sinuous aurora on nightside Mars, using images 130.4 and 135.6 nm oxygen emission measured by Emirates Mars Mission EMUS ultraviolet spectrograph, upstream measurements from MAVEN Express spacecraft. They are detected in ∼3% observations, totaling 73 clear detections. These emissions narrow, elongated (1,000–6,000 km), cross Mars' UV terminator, oriented generally toward anti‐solar point, clustering into north, south, east, west‐oriented...
Abstract Mars discrete aurorae are caused by accelerated electrons precipitating into the atmosphere and interacting with species such as atomic oxygen. However, energy of causing these remains currently unclear: no simultaneous concurrent measurements electron analyzers spectrometers have been performed so far, preventing from assessing exact downgoing auroral electrons. Several emissions observed far on Mars, among which two oxygen in ultraviolet at 130.4 135.6 nm. In this study, we...
We present a comprehensive study of the nightside aurora phenomenon on Mars, utilizing observations from EMUS onboard EMM. The oxygen emission at 130.4 nm is by far brightest FUV auroral line observed Mars. Our statistical analysis reveals geographic, solar zenith angle, local time, and seasonal dependencies occurrence. Higher occurrence in regions open magnetic topology, where crustal fields are either very weak or both strong vertical. Aurora occurs more frequently closer to terminator...
Abstract The Emirates Mars Ultraviolet Spectrometer (EMUS), aboard the Mission (EMM), has been conducting observations of ultraviolet emissions within Martian exosphere. Taking advantage distinctive orbit EMM around Mars, EMUS utilizes a dedicated strafe observation strategy to scan illuminated exosphere at tangential altitudes ranging from 130 over 20,000 km. To distinguish between origin and those interplanetary background, conducts specialized background by looking away planet. This...
Abstract We present a comprehensive study of the nightside aurora phenomenon on Mars, utilizing observations from EMUS onboard Emirates Mars Mission. The oxygen emission at 130.4 nm is by far brightest FUV auroral line observed Mars. Our statistical analysis reveals geographic, solar zenith angle, local time, and seasonal dependencies occurrence. Higher occurrence in regions open magnetic topology, where crustal fields are either very weak or both strong vertical. Aurora occurs more...
Abstract Water is lost from the Mars upper atmosphere to space as hydrogen and oxygen, both of which can be observed in scattered ultraviolet sunlight at 102.6 nm. We present Emirates Mission Ultraviolet Spectrometer (EMM/EMUS) insertion orbit observations this airglow, resolving independent altitude contributions H O for first time. airglow modeling complete nm system 3D azimuthally symmetric emission, retrieving temperatures densities typical northern spring. Our model reproduces emission...
We present a comprehensive study of the nightside discrete electron aurora phenomenon on Mars, utilizing observations from EMUS onboard EMM. The oxygen emission at 130.4 nm is by far brightest FUV auroral line observed Mars. identify pixels in OI disk observations, with higher sensitivity than previously possible. Our statistical analysis reveals regional, SZA, local time, and seasonal dependencies occurrence. Higher occurrence regions open magnetic topology vertical crustal fields. Aurora...
Benefiting from a large orbit and high sensitivity, the Emirates Mars mission EMUS instrument has provided first opportunity to synoptically regularly image Mars&#8217; discrete FUV auroral oxygen emission at 130.4 135.6 nm.&#160; Over 15-20 minutes, produces a) images by slewing its aperture slit across disk or b) &#8220;movies&#8221; of narrow regions staring continuously. Discrete aurora are observed primarily where magnetic topology is open (i.e. connected collisional...
Mars' lack of a global magnetic field led to initial expectations minimal auroral activity. Mars Express's SPICAM instrument nonetheless discovered an unusual form aurora in 2005. The ultraviolet emissions were confined near strong crustal region, showing that even weak fields can be responsible for aurora. These&#160;discrete&#160;aurora identified 19 observations over SPICAM's decade observations.&#160; MAVEN spacecraft arrived at 2014 carrying the Imaging UltraViolet...
We present a comprehensive study of the nightside discrete electron aurora phenomenon on Mars, utilizing observations from EMUS onboard EMM. The oxygen emission at 130.4 nm is by far brightest FUV auroral line observed Mars. identify pixels in OI disk observations, with higher sensitivity than previously possible. Our statistical analysis reveals regional, SZA, local time, and seasonal dependencies occurrence. Higher occurrence regions open magnetic topology vertical crustal fields. Aurora...
The Emirates Mars Ultraviolet Spectrometer (EMUS) onboard the Mission spacecraft, which observes ultraviolet emission between approximately 100 and 170 nm, has observed multiple instances of nightside aurora at Mars. Variations in auroral brightness morphology have been to change on timescales tens minutes. brightest aurorae are typically seen following space weather events, i.e., coronal mass ejection stream interaction region impacts. InSight Fluxgate Magnetometer (IFG) Interior...
One of the primary objectives Emirates Mars Mission (EMM) is to study seasonal variation upper atmosphere and associated changes in escape space. Here we present a preliminary analysis oxygen population inner exosphere (1.06-1.6 Martian radii) with nearly-contiguous sampling across all seasons from early MY 36 37. This thought be non-thermal photochemically generated driven by solar EUV, which can produce energetic atoms sufficient velocity Mars&#8217; gravity. The observations are made...
Discrete aurorae are produced by charged particle precipitation (mostly electrons) into the upper atmosphere. Electron impact causes electronic excitations of atoms and molecules in atmosphere, whose deexcitation releases ultraviolet photons. aurora was first discovered as an glow coming from &#8220;magnetic umbrellas&#8221; southern hemisphere. These strong crustal magnetic field regions on Mars, which remnants a global that decayed billions years ago. Both Mars Express (Bertaux et...
Atomic hydrogen and oxygen are the dominant species in Martian exosphere. is essentially produced from dissociation of H2O, whereas, hot atoms populated by non-thermal processes such as dissociative recombination O2+ with electrons ionosphere. The study these helps to understand evolution atmosphere more specifically history water on Mars.&#160; Emirates Mars Ultraviolet Spectrometer (EMUS), one primary instruments onboard Mission (EMM), has been observing atomic exosphere over Year 36....
Benefiting from a large orbit and high sensitivity, the Emirates Mars mission EMUS instrument has provided first opportunity to regularly image Mars&#8217; discrete FUV aurora synoptically.&#160; collected nearly 1000 synoptic observations of nightside have revealed at least three distinct types Aurora: 1) crustal field aurora, appearing in regions mostly radial magnetic fields, 2) patchy observed away strong 3) sinuous extending terminator typically thousands kilometers onto...
The surface of the planet Mars exhibits a record dessiccation and oxidation, legacy significant water escape to space as hydrogen oxygen. This H can be constrained using ultraviolet observations planet's upper atmosphere, where neutral atomic scatters UV sunlight. In time since its orbit insertion in early 2021, Emirates Ultraviolet Spectrometer (EMUS) on Mission (EMM) has been observing this at 102.6 nm 121.6 nm, Lyman beta alpha. Here we present rates retrieved from these observations,...
Traditionally, heliophysics is characterized as the study of near-Earth space environment, where plasmas and neutral gases originating from Earth Sun, to a lesser extent other solar system bodies, interact in ways that are detectable only through in-situ or close-range (usually within ~10 AU) remote sensing.As result, has data environment around handful objects, particular Sun Earth.Comparatively, Astrophysics an extensive array but more limited temporal, spatial, wavelength information any...
We present the first observations of dayside coronal oxygen emission in far ultraviolet (FUV) measured by Emirates Mars Ultraviolet Spectrometer (EMUS) onboard Mission (EMM).The high sensitivity EMUS is providing an opportunity to observe tenuous corona FUV, which otherwise difficult observe.Oxygen resonance fluorescence at 130.4 nm provides a measurement upper atmospheric and exospheric oxygen.471 profiles are constructed using long-exposure time cross-exospheric mode (OS4) observations.The...
&lt;p&gt;The Emirates Mars Ultraviolet Spectrometer (EMUS) instrument is one of three science instruments on board the &amp;#8220;Hope Probe&amp;#8221; Mission (EMM). EMM arrived at February 9 2021, in order to explore global dynamics Martian atmosphere, while sampling both diurnal and seasonal timescales. The EMUS a far-ultraviolet imaging spectrograph, jointly developed by Mohammed Bin Rashid Space Centre (MBRSC) Dubai, UAE Laboratory for Atmospheric Physics (LASP)...
&lt;p&gt;Here we report on synoptic (or &amp;#8220;disk&amp;#8221;) observations of Martian discrete aurora in the extreme and far ultraviolet (&lt;200 nm), made by Emirates Mars Ultraviolet Spectrometer (EMUS) board Mission (EMM). EMM is well-suited to studying due its high altitude vantage point regular observation cadence sensitivity EMUS instrument.&amp;#160; The first EUV/EUV auroral spectra measured at reveal O, C, CO features from 99 165 nm. Auroral detection...